  We investigate the formation of stars within giant molecular clouds (GMCs)
evolving in environments of different global magnetic field strength and
large-scale dynamics. Building upon a series of magnetohydrodynamic (MHD)
simulations of non-colliding and colliding GMCs, we employ density- and
magnetically-regulated star formation sub-grid models in clouds which range
from moderately magnetically supercritical to near critical. We examine gas and
star cluster morphologies, magnetic field strengths and relative orientations,
pre-stellar core densities, temperatures, mass-to-flux ratios and velocities,
star formation rates and efficiencies over time, spatial clustering of stars,
and kinematics of the stars and natal gas. The large scale magnetic criticality
of the region greatly affects the overall gas evolution and star formation
properties. GMC collisions enhance star formation rates and efficiencies in
magnetically supercritical conditions, but may actually inhibit them in the
magnetically critical case. This may have implications for star formation in
different Galactic environments such as the Galactic Center and the main
Galactic disk.
