  In a companion paper, we develop a theory for the evolution of stellar wind
driven bubbles in dense, turbulent clouds. This theory proposes that turbulent
mixing at a fractal bubble-shell interface leads to highly efficient cooling,
in which the vast majority of the input wind energy is radiated away. This
energy loss renders the majority of the bubble evolution momentum-driven rather
than energy-driven, with expansion velocities and pressures orders of magnitude
lower than in the classical Weaver77 solution. In this paper, we validate our
theory with three-dimensional, hydrodynamic simulations. We show that extreme
cooling is not only possible, but is generic to star formation in turbulent
clouds over more than three orders of magnitude in density. We quantify the few
free parameters in our theory, and show that the momentum exceeds the wind
input rate by only a factor ~ 1.2-4. We verify that the bubble/cloud interface
is a fractal with dimension ~ 2.5-2.7. The measured turbulent amplitude (v_t ~
200-400 km/s) in the hot gas near the interface is shown to be consistent with
theoretical requirements for turbulent diffusion to efficiently mix and radiate
away most of the wind energy. The fraction of energy remaining after cooling is
only 1-\Theta ~ 0.1-0.01, decreasing with time, explaining observations that
indicate low hot-gas content and weak dynamical effects of stellar winds.
