  We study the connection between the large-scale dynamics and the gas fueling
toward a central black hole via the analysis of a Milky Way-like simulation at
sub-parsec resolution. This allows us to follow a set of processes at various
scales (e.g., the triggering of inward gas motion towards inner resonances via
the large-scale bar, the connection to the central black hole via mini spirals)
in a self-consistent manner. This simulation provides further insights on the
role of shear for the inhibition of star formation within the bar in regions
with significant amount of gas. We also witness the decoupling of the central
gas and nuclear cluster from the large-scale disc, via interactions with the
black hole. This break of symmetry in the mass distribution triggers the
formation of gas clumps organised in a time-varying 250 pc ring-like structure,
the black hole being offset by about 70 pc from its centre. Some clumps form
stars, while most get disrupted or merge. Supernovae feedback further creates
bubbles and filaments, some of the gas being expelled to 100 pc or higher above
the galaxy plane. This helps remove angular momentum from the gas, which gets
closer to the central dark mass. Part of the gas raining down is being
accreted, forming a 10~pc polar disc-like structure around the black hole,
leading to an episode of star formation. This gives rise to multiple stellar
populations with significantly different angular momentum vectors, and may lead
to a natural intermittence in the fueling of the black hole.
