  We present a set of four Gemini-North GMOS/IFU observations of the central
disturbed regions of the dwarf irregular starburst galaxy NGC 1569, surrounding
the well-known super star clusters A and B. This continues on directly from a
companion paper, in which we describe the data reduction and analysis
techniques employed and present the analysis of one of the IFU pointings. By
decomposing the emission line profiles across the IFU fields, we map out the
properties of each individual component identified and identify a number of
relationships and correlations that allow us to investigate in detail the state
of the ionized ISM. Our observations support and expand on the main findings
from the analysis of the first IFU position, where we conclude that a broad (<
400 km/s) component underlying the bright nebular emission lines is produced in
a turbulent mixing layer on the surface of cool gas knots, set up by the impact
of the fast-flowing cluster winds. We discuss the kinematic, electron density
and excitation maps of each region in detail and compare our results to
previous studies. Our analysis reveals a very complex environment with many
overlapping and superimposed components, including dissolving gas knots,
rapidly expanding shocked shells and embedded ionizing sources, but no evidence
for organised bulk motions. We conclude that the four IFU positions presented
here lie well within the starburst region where energy is injected, and, from
the lack of substantial ordered gas flows, within the quasi-hydrostatic zone of
the wind interior to the sonic point. The net outflow occurs at radii beyond
100-200 pc, but our data imply that mass-loading of the hot ISM is active even
at the roots of the wind.
