  The molecular component of the Galaxy is comprised of turbulent, magnetized
clouds, many of which are self-gravitating and form stars. To understand how
these clouds' evolution may depend on their level of turbulence, mean
magnetization, and degree of self-gravity, we perform a survey of direct
numerical MHD simulations in 2.5 dimensions. Two of our independent survey
parameters allow us to model clouds which either meet or fail conditions for
magneto-Jeans stability and magnetic criticality. Our third survey parameter
allows us to initiate turbulence of either sub- or super-Alfv\'enic amplitude.
We evaluate the times for each cloud model to become gravitationally bound, and
measure each model's kinetic energy loss over the fluid flow crossing time. We
compare the evolution of density and magnetic field structural morphology, and
quantify the differences in the density contrast generated by internal
stresses, for models of differing mean magnetization. We find that the values
of (c_s/v_A)^2 and L/L_Jeans, but not the initial Mach number v/c_s, determine
the time for cloud gravitational binding and collapse. We find, contrary to
some previous expectations, less than a factor of two difference between
turbulent decay times for models with varying magnetic field strength. In all
models, we find turbulent amplification in the magnetic field strength, with
the turbulent magnetic energy between 25-60% of the turbulent kinetic energy
after one flow crossing time. We find that for non-self-gravitating stages of
evolution, the mass-averaged density contrast magnitudes <log(\rho/\bar\rho)>
are in the range 0.2-0.5; we note that only the more strongly-magnetized models
appear consistent with estimates of clump/interclump density contrasts inferred
in Galactic GMCs.
