The number of rich galaxy clusters per unit volume is a strong functio
n of Omega, the cosmological density parameter, and sigma(8), the line
ar extrapolation to z = 0 of the density contrast in 8 h(-1) Mpc spher
es. The Canadian Network for Observational Cosmology (CNOC) cluster re
dshift survey provides a sample of clusters, the average mass profiles
of which are accurately known, which enables a secure association bet
ween cluster numbers and the filtered density perturbation spectrum. W
e select from the CNOC cluster survey those Extended Medium-Sensitivit
y Survey clusters with bolometric L(x) greater than or equal to 10(45)
ergs s(-1) and a velocity dispersion exceeding 800 km s(-)1 in the re
dshift ranges 0.18-0.35 and 0.35-0.55. We compare the number density o
f these subsamples with similar samples at both high and low redshift.
Using the Press-Schechter formalism and cold dark matter (CDM) style
structure models, the density data are best described with sigma(8) si
milar or equal to 0.75 +/- 0.1 and Omega similar or equal to 0.4 +/- 0
.2 (90% confidence). The duster dynamical analysis gives Omega = 0.2 /- 0.1 for which sigma(8) = 0.95 +/- 0.1 (90% confidence). The predict
ed cluster density evolution in an Omega = 1 CDM model exceeds that ob
served by more than 1 order of magnitude.