  This work aims to derive the physical properties of the CNSFRs in the ring of
the face-on spiral NGC 7742 using IFS observations. We have selected 88
individual ionising clusters that power HII regions populating the ring of the
galaxy that may have originated in a minor merger event. For the HII regions
the rate of Lyman continuum photon emission is between 0.025 and 1.5 10$^{51}$
which points to these regions being ionised by star clusters. Their electron
density, ionisation parameter, filling factor and ionised hydrogen mass show
values consistent with those found in other studies of similar regions and
their metal abundances as traced by sulphur have been found to be between 0.25
and 2.4 times solar, with most regions showing values slightly below solar. The
equivalent temperature of the ionising clusters is relatively low, below 40000
K which is consistent with the high elemental abundances derived. The young
stellar population of the clusters has contributions of ionising and
non-ionising populations with ages around 5 Ma and 300 Ma respectively. The
masses of ionising clusters once corrected for the contribution of underlying
non-ionising populations were found to have a mean value of 3.5 $\times$ 10$^4$
M$_{\odot}$, comparable to the mass of ionised gas and about 20 \% of the
corrected photometric mass.
