  We present a detailed study of the kinematics of 19 QSO2s in the range
0.3<z<0.41 and [OIII] luminosities $L_{[OIII]} > 10^{8.5}$L$_{\odot}$. We aim
at advancing our understanding of the AGN feedback phenomenon by correlating
outflow properties with the presence of young stellar populations (YSPs) with
ages <100 Myr, the optical morphology and the environment of the galaxies, and
the radio luminosity.
  We characterize the ionized gas kinematics using the
[OIII]$\lambda$5007$\r{A}$ profiles, through three different outflow detection
methods: multi-component parametric and flux-weighted and peak-weighted
non-parametric.
  We detect ionized outflows in 18 QSO2s using the parametric analysis, and in
all of them using the non-parametric methods. We find higher outflow masses
using the parametric analysis (log M$_{OF}$(M$_{\odot}$)=6.47$\pm$0.50), and
larger mass rates and kinetic powers with the flux-weighted non-parametric
method (\.M$_{OF}$=4.0$\pm$4.4 M$_{\odot}$ yr$^{-1}$ and
log(\.E$_{kin}$)=41.9$\pm$0.6 erg~s$^{-1}$). However, it is when we use the
parametric method and the maximum outflow velocities that we measure the
highest outflow mass rates and kinetic energies (23$\pm$35 M$_{\odot}$
yr$^{-1}$ and 42.9$\pm$0.6 erg s$^{-1}$). We do not find any significant
correlation between the outflow properties and the previously mentioned galaxy
properties.
  4 out of 5 QSO2s without a YS<100 Myr show highly disturbed kinematics,
whereas only 5 out of the 14 QSO2s with YSPs show similarly asymmetric [OIII]
profiles. This might be indicative of negative feedback. The lack of
correlation between the outflow properties and the presence of mergers in
different interaction stages might be due to their different dynamical
timescales. Lastly, the small radio luminosity range covered by our sample may
be impeding the detection of any correlation between radio emission and outflow
properties.
