  The systematic errors in the virial mass-to-light ratio, M_v/L, of galaxy
clusters as an estimator of the field M/L value are assessed. We overlay 14
clusters in redshift space to create an ensemble cluster which averages over
substructure and asymmetries. The combined sample, including background,
contains about 1150 galaxies, extending to a projected radius of about twice
r_200. The radius r_200, defined as where the mean interior density is 200
times the critical density, is expected to contain the bulk of the virialized
cluster mass. The dynamically derived M(r_200)/L(r_200) of the ensemble is
0.82+/-0.14 <M_v/L>. The M_v/L overestimate is attributed to not taking into
account the surface pressure term in the virial equation. Under the assumption
that the velocity anisotropy parameter is in the range 0<=\beta<=2/3, the
galaxy distribution accurately traces the mass profile beyond about the central
0.3r_200. There are no color or luminosity gradients in the galaxy population
beyond 2r_200, but there is 0.11+/-0.05 mag fading in the r band luminosities
between the field and cluster galaxies. We correct the cluster virial
mass-to-light ratio, M_v/L=289+/-50 h\msun/\lsun (calculated assuming q_0=0.1),
for the biases in M_v and mean luminosity to estimate the field M/L=213+/-59
h\msun/\lsun. With our self-consistently derived field luminosity density,
j/\rho_c=1136+/-138 h\msun/\lsun (at z~1/3), the corrected M/L indicates
\Omega_0=0.19+/-0.06+/-0.04 (formal 1\sigma random error and estimated
potential systematic errors).
