  The origin of the observed morphological and kinematic substructure of young
star forming regions is a matter of debate. We offer a new analysis of data
from simulations of globally gravitationally collapsing clouds of progenitor
gas to answer questions about sub-structured star formation in the context of
cold collapse. As a specific example, we compare our models to recent radial
velocity survey data from the IN-SYNC survey of Orion and new observations of
dense gas kinematics, and offer possible interpretations of kinematic and
morphological signatures in the region. In the context of our model, we find
the frequently-observed hub-filament morphology of the gas naturally arises
during gravitational evolution, as well as the dynamically-distinct kinematic
substructure of stars. We emphasize that the global and not just the local
gravitational potential plays an important role in determining the dynamics of
both clusters and filaments.
