  Galaxies comprise intricate networks of interdependent processes which
together govern their evolution. Central among these are the multiplicity of
feedback channels, which remain incompletely understood. One outstanding
problem is the understanding and modeling of the multiphase nature of galactic
winds, which play a crucial role in galaxy formation and evolution. We present
the results of three dimensional magnetohydrodynamical tall box interstellar
medium patch simulations with clustered supernova driven outflows.
Fragmentation of the interstellar medium during superbubble breakout seeds the
resulting hot outflow with a population of cool clouds. We focus on analyzing
and modeling the origin and properties of these clouds. Their presence induces
large scale turbulence, which in turn leads to complex cloud morphologies.
Cloud sizes are well described by a power law distribution and mass growth
rates can be modelled using turbulent radiative mixing layer theory. Turbulence
provides significant pressure support in the clouds, while magnetic fields only
play a minor role. We conclude that many of the physical insights and analytic
scalings derived from idealized small scale simulations translate well to
larger scale, more realistic turbulent magnetized winds, thus paving a path
towards their necessary yet challenging inclusion in global-scale galaxy
models.
