  There is now abundant observational evidence that star formation is a highly
dynamical process that connects filament hierarchies and supernova feedback
from galaxy scale kpc filaments and superbubbles, to giant molecular clouds
(GMCs) on 100 pc scales and star clusters (1 pc). Here we present galactic
multi-scale MHD simulations that track the formation of structure from galactic
down to sub pc scales in a magnetized, Milky Way like galaxy undergoing
supernova driven feedback processes. We do this by adopting a novel zoom-in
technique that follows the evolution of typical 3-kpc sub regions without
cutting out the surrounding galactic environment, allowing us to reach 0.28 pc
resolution in the individual zoom-in regions. We find a wide range of
morphologies and hierarchical structure including superbubbles, turbulence, kpc
atomic gas filaments hosting multiple GMC condensations that are often
associated with superbubble compression; down to smaller scale filamentary GMCs
and star cluster regions within them. Gas accretion and compression ultimately
drive filaments over a critical, scale - dependent, line mass leading to
gravitational instabilities that produce GMCs and clusters. In quieter regions,
galactic shear can produce filamentary GMCs within flattened, rotating
disk-like structures on 100 pc scales. Strikingly, our simulations demonstrate
the formation of helical magnetic fields associated with the formation of these
disk like structures.
