Interactions between dense clumps in molecular cloud complexes are discussed. Two types of clump motions are envisioned: orbital-type motions, where the average relative velocity between clumps approximately equals the observed cloud linewidth, and magnetically-constrained turbulence, where the relative velocities between near-neighbor clumps can be much less than the cloud linewidth. Various
... [Show full abstract] observations that could distinguish between these possibilities are proposed. The empirical correlations observed for molecular clouds are attributed to virialized motions in a constant pressure environment. A simple model of supersonic clump interactions is used to identify possible states of turbulent pressure equilibrium.