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The IRDC G14.225-0.506 is associated with a network of filaments, whichresult in two different dense hubs, as well as with several signposts of starformation activity. The aim of this work is to study the cm continuum emissionto characterize the stellar population in G14.2. We performed deep (~1.5-3microJy) radio continuum observations at 6 and 3.6 cm using the VLA in the Aconfiguration (~0.3''). We have also made use of observations taken duringdifferent days to study the presence of variability at short timescales. Wedetected a total of 66 sources, 32 in the northern region G14.2-N and 34 in thesouthern region G14.2-S. Ten of the sources are found to be variable. Based ontheir spectral index, the emission in G14.2-N is mainly dominated bynon-thermal sources while G14.2-S contains more thermal emitters. Approximately75% of the sources present a counterpart at other wavelengths. In the inner0.4~pc region around the center of each hub, the number of IR sources inG14.2-N is larger than in G14.2-S by a factor of 4. We also studied therelation between the radio luminosity and the bolometric luminosity, findingthat the thermal emission of the studied sources is compatible with thermalradio jets. For our sources with X-ray counterparts, the non-thermal emittersfollow a G\"udel-Benz relation with k = 0.03. We found similar levels offragmentation between G14.2-N and G14.2-S, suggesting that both regions aremost likely twin hubs. The non-thermal emission found in the less evolvedobjects suggests that G14.2-N may be composed of more massive YSOs as well asbeing in a more advanced evolutionary stage, consistent with the filament-halogradient in age and mass from previous works. Our results confirm a widerevolutionary sequence starting in G14.2-S as the youngest part, followed byG14.2-N, and ending with the most evolved region M17.

Radio survey of the stellar population in the infrared dark cloud G14.225-0.506