  Stellar winds contain enough energy to easily disrupt the parent cloud
surrounding a nascent star cluster, and for this reason have been considered
candidates for regulating star formation. However, direct observations suggest
most wind power is lost, and Lancaster21a,b recently proposed that this is due
to efficient mixing and cooling processes. Here, we simulate star formation
with wind feedback in turbulent, self-gravitating clouds, extending our
previous work. Our simulations cover clouds with initial surface density
$10^2-10^4$ $M_{\odot} \, {\rm pc}^{-2}$, and show that star formation and
residual gas dispersal is complete within 2 - 8 initial cloud free-fall times.
The "Efficiently Cooled" model for stellar wind bubble evolution predicts
enough energy is lost for the bubbles to become momentum-driven, we find this
is satisfied in our simulations. We also find that wind energy losses from
turbulent, radiative mixing layers dominate losses by "cloud leakage" over the
timescales relevant for star formation. We show that the net star formation
efficiency (SFE) in our simulations can be explained by theories that apply
wind momentum to disperse cloud gas, allowing for highly inhomogeneous internal
cloud structure. For very dense clouds, the SFE is similar to those observed in
extreme star-forming environments. Finally, we find that, while self-pollution
by wind material is insignificant in cloud conditions with moderate density
(only $\lesssim 10^{-4}$ of the stellar mass originated in winds), our
simulations with conditions more typical of a super star cluster have star
particles that form with as much as 1\% of their mass in wind material.
