  Radio Active Galactic Nuclei (RAGN) are found preferentially in dense
structures (i.e., clusters/groups) at redshifts of z$<$2 and are commonly used
to detect protoclusters at higher redshift. Here, we attempt to study the host
and environmental properties of two relatively faint ($\mathrm
L_\mathrm{1.4GHz} \sim10^{25}$ W Hz$^{-1}$) RAGN in a known protocluster at
z=3.3 in the PCl J0227-0421 field, detected using the latest radio observation
obtained as part of the ORELSE Survey. Using new spectroscopic observations
obtained from Keck/MOSFIRE as part of the Charting Cluster Construction with
VUDS and ORELSE (C3VO) survey and previous spectroscopic data obtained as part
of the VIMOS-VLT Deep Survey (VVDS) and VIMOS Ultra-Deep Survey (VUDS), we
revise the three-dimensional overdensity field around this protocluster. The
protocluster is embedded in a large scale overdensity proto-structure. This
proto-structure has an estimated total mass of $\sim2.6\times10^{15}$ M$_\odot$
and contains several overdensity peaks. Both RAGN are hosted by very bright and
massive galaxies, while their hosts show extreme differences color, indicating
that they have different ages and are in different evolutionary stages.
Furthermore, we find that they are not in the most locally dense parts of the
proto-structure, but are fairly close to the centers of their parent
overdensity peaks. We propose a scenario where merging might already have
happened in both cases that have lowered the local density of their surrounding
area and boosted their stellar mass. This work is the first time that two RAGN
at low-luminosity have been found and studied within a high redshift
proto-structure.
