  Using K-band imaging for 15 of the Canadian Network for Observational
Cosmology (CNOC1) clusters we examine the near-infrared properties of
moderate-redshift (0.19 < z < 0.55) galaxy clusters. We find that the number of
K-band selected cluster galaxies within R_{500} (the Halo Occupation Number,
HON) is well-correlated with the the cluster dynamical mass (M_{500}) and X-ray
Temperature (T_{x}); however, the intrinsic scatter in these scaling relations
is 37% and 46% respectively. Comparison with clusters in the local universe
shows that the HON-M_{500} relation does not evolve significantly between z = 0
and z ~ 0.3. This suggests that if dark matter halos are disrupted or undergo
significant tidal-stripping in high-density regions as seen in numerical
simulations, the stellar mass within the halos is tightly bound, and not
removed during the process. The total K-band cluster light (L_{200,K}) and
K-band selected richness (parameterized by B_{gc,K}) are also correlated with
both the cluster T_{x} and M_{200}. The total (intrinsic) scatter in the
L_{200,K}-M_{200} and B_{gc,K}-M_{200} relations are 43%(31%) and 35%(18%)
respectively and indicates that for massive clusters both L_{200,K} and
B_{gc,K} can predict M_{200} with similar accuracy as T_{x}, L_{x} or optical
richness (B_{gc}). Examination of the mass-to-light ratios of the clusters
shows that similar to local clusters, the K-band mass-to-light ratio is an
increasing function of halo mass. Using the K-band mass-to-light ratios of the
clusters, we apply the Oort technique and find Omega_{m,0} = 0.22 pm 0.02,
which agrees well with recent combined concordance cosmology parameters, but,
similar to previous cluster studies, is on the low-density end of preferred
values.
