  Winds from young massive stars contribute a large amount of energy to their
host molecular clouds. This has consequences for the dynamics and observable
structure of star-forming clouds. In this paper, we present radiative
magnetohydrodynamic simulations of turbulent molecular clouds that form
individual stars of 30, 60 and 120 solar masses emitting winds and ultraviolet
radiation following realistic stellar evolution tracks. We find that winds
contribute to the total radial momentum carried by the expanding nebula around
the star at 10 % of the level of photoionisation feedback, and have only a
small effect on the radial expansion of the nebula. Radiation pressure is
largely negligible in the systems studied here. The 3D geometry and evolution
of wind bubbles is highly aspherical and chaotic, characterised by fast-moving
"chimneys" and thermally-driven "plumes". These plumes can sometimes become
disconnected from the stellar source due to dense gas flows in the cloud. Our
results compare favourably with the findings of relevant simulations, analytic
models and observations in the literature while demonstrating the need for full
3D simulations including stellar winds. However, more targeted simulations are
needed to better understand results from observational studies.
