  We study the formation and early evolution of star clusters that have a wide
range of masses and background cloud mass surface densities, $\Sigma_{\rm
cloud}$, which help set the initial sizes, densities, and velocity dispersions
of the natal gas clumps. Initial clump masses of 300, $3,000$ and $30,000$
$M_\odot$ are considered, from which star clusters are born with an assumed 50%
overall star formation efficiency and with 50% primordial binarity. This
formation is gradual, i.e., with a range of star formation efficiencies per
free-fall time from 1% to 100%, so that the formation time can range from 0.7
Myr for low-mass, high-$\Sigma_{\rm cloud}$ clumps to $\sim30$ Myr for
high-mass, low-$\Sigma_{\rm cloud}$ clumps. Within this framework of the
Turbulent Clump model, for a given $\Sigma_{\rm cloud}$, clumps of higher mass
are of lower initial volume density, but their dynamical evolution leads to
higher bound fractions and causes them to form much higher density cluster
cores and maintain these densities for longer periods. This results in
systematic differences in the evolution of binary properties, degrees of mass
segregation and rates of creation of dynamically ejected runaways. We discuss
the implications of these results for observed star clusters and stellar
populations.
