We have measured velocity dispersions for a sample of 36 galaxies with J < 21.2 or Mr < -20.6 mag in MS1054-03, a massive cluster of galaxies at z = 0.83. Our data are of uniformly high quality down to our selection limit, our 16-hour exposures typically yielding errors of only delta(dispersion)~10% for L* and fainter galaxies. By combining our measurements with data from the literature, we have 53 cluster galaxies with measured dispersions, and HST/ACS-derived sizes, colors and surface brightnesses. This sample is complete for the typical L* galaxy at z~1, unlike most previous z~1 cluster samples which are complete only for the massive cluster members (>1e11 M_sun). We find no evidence for a change in the tilt of the fundamental plane (FP). Nor do we find evidence for evolution in the slope of the color-dispersion relation and M/L_B-dispersion relations; measuring evolution at a fixed dispersion should minimize the impact of size evolution found in other work. The M/L_B at fixed dispersion evolves by Delta log10 M/L_B=-0.50 +/- 0.03 between z=0.83 and z=0.02 or d(log10 M/L_B)=-0.60 +/- 0.04 dz, and we find Delta (U-V)_z=-0.24 +/- 0.02 mag at fixed dispersion in the rest-frame, matching the expected evolution in M/L_B within 2.25 standard deviations. The implied formation redshift from both the color and M/L_B evolution is z*=2.0 +/- 0.2 +/- 0.3 (sys), during the epoch in which the cosmic star-formation activity peaked, with the systematic uncertainty showing the dependence of z* on the assumptions we make about the stellar populations. The lack of evolution in either the tilt of the FP or in the M/L- and color-dispersion relations imply that the formation epoch depends weakly on mass, ranging from z*=2.3 +1.3 -0.3 at 300 km/s to z*=1.7 +0.3 -0.2 at 160 km/s and implies that the IMF similarly varies slowly with galaxy mass.
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