  We investigate collisions between giant molecular clouds (GMCs) as potential
generators of their internal turbulence. Using magnetohydrodynamic (MHD)
simulations of self-gravitating, magnetized, turbulent, GMCs, we compare
kinematic and dynamic properties of dense gas structures formed when such
clouds collide compared to those that form in non-colliding clouds as
self-gravity overwhelms decaying turbulence. We explore the nature of
turbulence in these structures via distribution functions of density, velocity
dispersions, virial parameters, and momentum injection. We find that the dense
clumps formed from GMC collisions have higher effective Mach number, greater
overall velocity dispersions, sustain near-virial equilibrium states for longer
times, and are the conduit for injection of turbulent momentum into high
density gas at high rates.
