  With its sensitivity in the rest-frame optical, the James Webb Space
Telescope (JWST) has uncovered active galactic nuclei (AGN), comprising both
intrinsically faint and heavily reddened sources, well into the first billion
years of the Universe, at $z \sim 4-11$. In this work, we revisit the AGN
contribution to reionization given the high number densities associated with
these objects. We use the DELPHI semi-analytic model, base-lined against the
latest high-redshift datasets from the JWST and the Atacama Large millimetre
Array (ALMA) to model early star forming galaxies and AGN. We calculate the
escape fractions of ionizing radiation from both star formation and AGN and
include the impact of reionization feeback in suppressing the baryonic content
of low-mass galaxies in ionized regions. This model is validated against the
key observables for star forming galaxy, AGN and reionization. In our {\it
fiducial} model, reionization reaches its mid-point at $z \sim 6.9$ and ends by
$z \sim 5.9$. Low stellar mass ($M_*\leq 10^9M_\odot$) star forming galaxies
are found to be the key drivers of the reionization process, providing about
$77\%$ of the total photon budget. Despite their high numbers, high accretion
rates and higher escape fractions compared to star forming galaxies at $z \sim
5$, AGN only provide about $23\%$ of the total reionization budget which is
dominated by black holes in high stellar mass systems (with $M_* \geq
10^9M_\odot$). This is because AGN number densities become relevant only at $z
\leq 7$ - as a result, AGN contribute as much as galaxies as late as $z \sim
6.2$, when reionization is already in its end stages. Finally, we find that
even contrasting models of the AGN ionizing photon escape fraction (increasing
or decreasing with stellar mass) do not qualitatively change our results.
