  Star formation is a clustered process that regulates the structure and
evolution of galaxies. We investigate this process in the dwarf galaxy Haro 11,
forming stars in three knots (A, B, C). The exquisite resolution of HST imaging
allows us to resolve the starburst into tens of bright star clusters. We derive
masses between $10^5$ and $10^7\,\rm M_{\odot}$ and ages younger than 20 Myr,
using photometric modeling. We observe that the clustered star formation has
propagated from knot C (the oldest) through knot A (in between) towards knot B
(the youngest). We use aperture-matched ultraviolet and optical spectroscopy
(HST + MUSE) to independently study the stellar populations of Haro 11 and
determine the physical properties of the stellar populations and their feedback
in 1 kpc diameter regions. We discuss these results in light of the properties
of the ionised gas within the knots. We interpret the broad blue-shifted
components of the optical emission lines as outflowing gas ($v_{max} \sim 400$
km/s). The strongest outflow is detected in knot A with a mass-rate of
$\dot{M}_{out}\sim 10\,\rm M_{\odot}/yr$, ten times higher than the
star-formation in the same region. Knot B hosts a young and not fully developed
outflow, whereas knot C has likely been already evacuated. Because Haro 11 has
properties similar to high-redshift unresolved galaxies, our work can
additionally aid the understanding of star formation at high redshift, a window
that will be opened by upcoming facilities.
