  The IRDC G14.225-0.506 is associated with a network of filaments, which
result in two different dense hubs, as well as with several signposts of star
formation activity. The aim of this work is to study the cm continuum emission
to characterize the stellar population in G14.2. We performed deep (~1.5-3
microJy) radio continuum observations at 6 and 3.6 cm using the VLA in the A
configuration (~0.3''). We have also made use of observations taken during
different days to study the presence of variability at short timescales. We
detected a total of 66 sources, 32 in the northern region G14.2-N and 34 in the
southern region G14.2-S. Ten of the sources are found to be variable. Based on
their spectral index, the emission in G14.2-N is mainly dominated by
non-thermal sources while G14.2-S contains more thermal emitters. Approximately
75% of the sources present a counterpart at other wavelengths. In the inner
0.4~pc region around the center of each hub, the number of IR sources in
G14.2-N is larger than in G14.2-S by a factor of 4. We also studied the
relation between the radio luminosity and the bolometric luminosity, finding
that the thermal emission of the studied sources is compatible with thermal
radio jets. For our sources with X-ray counterparts, the non-thermal emitters
follow a G\"udel-Benz relation with k = 0.03. We found similar levels of
fragmentation between G14.2-N and G14.2-S, suggesting that both regions are
most likely twin hubs. The non-thermal emission found in the less evolved
objects suggests that G14.2-N may be composed of more massive YSOs as well as
being in a more advanced evolutionary stage, consistent with the filament-halo
gradient in age and mass from previous works. Our results confirm a wider
evolutionary sequence starting in G14.2-S as the youngest part, followed by
G14.2-N, and ending with the most evolved region M17.
