We report and discuss high-resolution echelle spectra of more than 100 F, G, and K dwarfs in the Pleiades. Comparisons of the profiles of Halpha and the Ca II infrared triplet to chromospherically inactive field stars allow us to measure chromospheric activity in these stars, and we have determined v sin i values to a limit of 7 km s-1. We have combined these new observations with published data and have conducted a census to assess the state of our knowledge of Pleiades solar-type stars. After allowing for a patch of heavy reddening in the southwest part of the cluster, consistent dereddened colors are determined from the available photometry and temperatures are derived. Rotation is fully resolved in the Pleiades for stars more massive than the Sun, but for less massive stars there are still too many upper limits to v sin i to determine the underlying, intrinsic distribution of rotation. Over the entire mass range we consider (1.4 greater than or similar to M / M. greater than or similar to 0.6), no single value can characterize rotation at any one mass because the spread is too large. Most G and K dwarfs in the Pleiades rotate slowly (v sin i less than or similar to 10 km s-1), but approximately 20% of the stars are ultrafast rotators (UFRs) with v sin i greater than or similar to 30 km s-1. That fraction of UFRs is independent of color, and the highest rotation rates are found among the K dwarfs. The surfaces of the many slowly rotating solar-type stars in the Pleiades are already rotating at or near the rate of stars of the same mass in the Hyades. That means that the dominant aspect of the evolution of rotation from the age of the Pleiades to the Hyades is convergence in rotation. Among the F dwarfs, the degree of convergence is about a factor of 5, but among the K stars it is at least a factor of 20. We argue that this convergence, as well as the large number of slow rotators at 1.0 M. suggests that the convective envelopes and radiative cores of these Pleiads are rotationally decoupled, with later replenishment of angular momentum to the envelope. The Pleiades also shows a broad range in the strength of chromospheric emission (CE) at any one color. CE depends on both mass and rotation, but, once the rotation is normalized to an index akin to the Rossby number, rotation and activity are well correlated. Most G and K dwarfs in the Pleiades show Halpha and the infrared triplet in absorption, with filling in of the line cores. Some stars show overt Halpha emission comparable in strength and profile to the weaker T Tauri stars, and a few even show overt emission at the infrared triplet. We have also found three G dwarfs with peculiar Halpha profiles whose rotation rates substantially exceed those seen previously in the Pleiades among stars of their color. These stars show very broad wings to their Halpha emission profiles, suggesting that the emission arises over a broad range of height in the stars' atmospheres.
