  Massive protostars attain high luminosities as they are actively accreting
and the radiation pressure exerted on the gas in the star's atmosphere may
launch isotropic high-velocity winds. These winds will collide with the
surrounding gas producing shock-heated ($T\sim 10^7$ K) tenuous gas that
adiabatically expands and pushes on the dense gas that may otherwise be
accreted. We present a suite of 3D radiation-magnetohydrodynamic simulations of
the collapse of massive prestellar cores and include radiative feedback from
the stellar and dust-reprocessed radiation fields, collimated outflows, and,
for the first time, isotropic stellar winds to model how these processes affect
the formation of massive stars. We find that winds are initially launched when
the massive protostar is still accreting and its wind properties evolve as the
protostar contracts to the main-sequence. Wind feedback drives asymmetric
adiabatic wind bubbles that have a bipolar morphology because the dense
circumstellar material pinches the expansion of the hot shock-heated gas. We
term this the "wind tunnel effect." If the core is magnetized, wind feedback is
less efficient at driving adiabatic wind bubbles initially because magnetic
tension delays their growth. We find that wind feedback eventually quenches
accretion onto $\sim$30 $\rm{M_{\rm \odot}}$ protostars that form from the
collapse of the isolated cores simulated here. Hence, our results suggest that
$\gtrsim$30 $\rm{M_{\rm \odot}}$ stars likely require larger-scale dynamical
inflows from their host cloud to overcome wind feedback. Additionally, we
discuss the implications of observing adiabatic wind bubbles with
\textit{Chandra} while the massive protostars are still highly embedded.
