  It has long been discussed whether stellar feedback in the form of winds
and/or radiation can shred the nascent molecular cloud, thereby controlling the
star formation rate. However, directly probing and quantifying the impact of
stellar feedback on the neutral gas of the nascent clouds is challenging. We
present an investigation doing exactly that toward the RCW 79 HII region using
the ionized carbon line at 158 $\mu$m ([CII]) from the FEEDBACK Legacy Survey.
We combine this data with information on the dozen ionizing O stars responsible
for the evolution of the region, and observe in [CII] for the first time both
blue- and red-shifted mostly neutral high-velocity gas which reaches velocities
up to 25 km s$^{-1}$ relative to the bulk emission of the molecular cloud. This
high-velocity gas mostly contains neutral gas and partly forms a fragmented
shell, similar to recently found shells in a few Galactic HII regions. However,
this shell does not account for all of the observed neutral high-velocity gas.
We also find high-velocity gas streaming out of the nascent cloud through holes
and obtain a range of dynamical timescales below 1.0 Myr for the high-velocity
gas which is well below the 2.3$\pm$0.5 Myr age of the OB cluster. This
suggests a different scenario for the evolution of RCW 79, where the
high-velocity gas is not solely stemming from a spherical expanding bubble, but
also from gas recently ablated at the edge of the turbulent molecular cloud
into the surrounding interstellar medium through low-pressure holes or
chimneys. The resulting mass ejection rate estimate for the cloud is
0.9-3.5$\times$10$^{-2}$ M$_{\odot}$~yr$^{-1}$, which leads to short erosion
timescales, i.e. $<$5 Myr, for the nascent molecular cloud. This finding
provides direct observational evidence of rapid molecular cloud dispersal.
