  The redshift evolution of the galaxy two-point correlation function is a
fundamental cosmological statistic. To identify similar galaxy populations at
different redshifts, we select a strict volume-limited sample culled from the
6100 cataloged CNOC2 galaxies. Our high-luminosity subsample selects galaxies
having k-corrected and evolution-compensated R luminosities, M_R^{k,e}, above
-20 mag (H_0=100 km/s/Mpc) where M_ast^{k,e}(R)simeq -20.3 mag. This subsample
contains about 2300 galaxies distributed between redshifts 0.1 and 0.65 spread
over a total of 1.55 square degrees of sky. A similarly defined low-redshift
sample is drawn from the Las Campanas Redshift Survey. We find that the
co-moving two-point correlation function can be described as xi(r|z) =
(r_00/r)^gamma (1+z)^{-(3+epsilon-gamma)} with r_{00}=5.03+/-0.08/h Mpc,
epsilon=-0.17+/- 0.18 and gamma=1.87+/-0.07 over the z=0.03 to 0.65 redshift
range, for Omega_M=0.2, Lambda=0. The measured clustering amplitude and its
evolution are dependent on the adopted cosmology. The measured evolution rates
for Omega_M=1 and flat Omega_M=0.2 background cosmologies are
epsilon=0.80+/-0.22 and epsilon=-0.81+/-0.19, respectively, with r_{00} of
5.30+/-0.1/h Mpc and 4.85+/-0.1/h Mpc, respectively. The sensitivity of the
derived correlations to the evolution corrections and details of the
measurements is presented. The analytic prediction of biased clustering
evolution for only the low density, LambdaCDM cosmology is readily consistent
with the observations, with biased clustering in an open cosmology somewhat
marginally excluded and a biased Omega_M=1 model predicting clustering
evolution that is more than 6 standard deviations from the measured value.
