  We present [CII] 158 $\mu$m and [OI] 63 $\mu$m observations of the bipolar
HII region RCW 36 in the Vela C molecular cloud, obtained within the SOFIA
legacy project FEEDBACK, which is complemented with APEX $^{12/13}$CO(3-2) and
Chandra X-ray (0.5-7 keV) data. This shows that the molecular ring, forming the
waist of the bipolar nebula, expands with a velocity of 1 - 1.9 km s$^{-1}$. We
also observe an increased linewidth in the ring indicating that turbulence is
driven by energy injection from the stellar feedback. The bipolar cavity hosts
blue-shifted expanding [CII] shells at 5.2$\pm$0.5$\pm$0.5 km s$^{-1}$
(statistical and systematic uncertainty) which indicates that expansion out of
the dense gas happens non-uniformly and that the observed bipolar phase might
be relatively short ($\sim$0.2 Myr). The X-ray observations show diffuse
emission that traces a hot plasma, created by stellar winds, in and around RCW
36. At least 50 \% of the stellar wind energy is missing in RCW 36. This is
likely due to leakage which is clearing even larger cavities around the bipolar
RCW 36 region. Lastly, the cavities host high-velocity wings in [CII] which
indicates relatively high mass ejection rates ($\sim$5$\times$10$^{-4}$
M$_{\odot}$ yr$^{-1}$). This could be driven by stellar winds and/or radiation
pressure, but remains difficult to constrain. This local mass ejection, which
can remove all mass within 1 pc of RCW 36 in 1-2 Myr, and the large-scale
clearing of ambient gas in the Vela C cloud indicates that stellar feedback
plays a significant role in suppressing the star formation efficiency (SFE).
