  The electromagnetic emission and the afterglow observations of the binary
neutron star merger event GW 170817A confirmed the association of the merger
with a short gamma-ray burst (sGRB) harboring a narrow ($5${\deg}-$10${\deg})
and powerful ($10^{49}$-$10^{50}~$erg) jet. Using the 1~second-long
neutrino-radiation-GR-MHD simulation of coalescing neutron stars of Kiuchi et
al. (2023) and following the semi-analytical estimates of Pais et al. (2023),
we inject a narrow, powerful, unmagnetized jet into the post-merger phase. We
explore different opening angles, luminosities, central engine durations, and
times after the merger. We explore early ($0.1~$s following the merger) and
late ($1~$s) jet launches; the latter is consistent with the time delay of
$\approx 1.74~$s observed between GW 170817 and GRB 170817A. We demonstrate
that the semi-analytical estimates correctly predict the jets' breakout and
collimation conditions. When comparing our synthetic afterglow light curves to
the observed radio data of GW170807, we find a good agreement for a $3 \times
10^{49}$ ergs jet launched late with an opening angle in the range $\simeq
5${\deg}-$7${\deg}.
