  The time-scales associated with various stages of the star formation process
represent major unknowns in our understanding of galactic evolution, as well as
of star and planet formation. This is the second paper in a series aiming to
establish a multi-tracer time-line of star formation in the Large Magellanic
Cloud (LMC), focusing on the lifecycle of molecular clouds. We use a
statistical method to determine a molecular cloud lifetime in the LMC of
$t_{\text{CO}}=11.8^{+2.7}_{-2.2}$ Myr. This short time-scale is similar to the
cloud dynamical time, and suggests that molecular clouds in the LMC are largely
decoupled from the effects of galactic dynamics and have lifetimes set by
internal processes. This provides a clear contrast to atomic clouds in the LMC,
of which the lifetimes are correlated with galactic dynamical time-scales. We
additionally derive the time-scale for which molecular clouds and HII regions
co-exist as $t_{\text{fb}}=1.2^{+0.3}_{-0.2}$ Myr, implying an average feedback
front expansion velocity of 12 km s$^{-1}$, consistent with expansion
velocities of HII regions in the LMC observed directly using optical
spectroscopy. Taken together, these results imply that the molecular cloud
lifecycle in the LMC proceeds rapidly and is regulated by internal dynamics and
stellar feedback. We conclude by discussing our measurements in the context of
previous work in the literature, which reported considerably longer lifetimes
for molecular clouds in the LMC, and find that these previous findings resulted
from a subjective choice in timeline calibration that is avoided by our
statistical methodology.
