  The CNOC2 field galaxy redshift survey is designed to provide measurements of
the evolution of galaxies and their clustering over the redshift range 0 to
0.7. The sample is spread over four sky patches with a total area of about 1.5
square degrees. Here we report preliminary results based on two of the sky
patches, and the redshift range of 0.15 to 0.55. We find that galaxy evolution
can be statistically described as nearly pure luminosity evolution of early and
intermediate SED types, and nearly pure density evolution of the late SED
types. The correlation of blue galaxies relative to red galaxies is similar on
large scales but drops by a factor of three on scales less than about 0.3/h
mpc, approximately the mean scale of virialization. There is a clear, but
small, 60%, change in clustering with 1.4 mag of luminosity. To minimize these
population effects in our measurement of clustering evolution, we choose
galaxies with M_r^{k,e}<= -20 mag as a population whose members are most likely
to be conserved with redshift. Remarkably, the evolution of the clustered
density in proper co-ordinates at r < 10/h Mpc, proportional to r_0^gamma
(1+z)^3, is best described as a ``de-clustering'', (1+z)^{0.6+/-0.4}. Or
equivalently, there is a weak growth of clustering in co-moving co-ordinates,
x_0~ (1+z)^{-0.3 +/- 0.2}. This conclusion is supported by the pairwise
peculiar velocities which rise slightly, but not significantly, into the past.
The Cosmic Virial Theorem applied to the CNOC2 data gives Q Omega_M/b=0.11 +/-
0.04$, where Q is the three point correlation parameter and b the bias.
Similarly, galaxy groups have a virial mass-to-light ratio (evolution
corrected) of M_{virial}/L_R^{k,e} = 215h Lsun/Msun, or Omega_M=0.15 +/- 0.05.
