  We present a multi-frequency (144 MHz - 9 GHz) and multi-scale (5 pc - 50
kpc) investigation of the central radio galaxy in RBS 797, by means of JVLA,
LOFAR (with international stations), e-Merlin, VLBA and EVN data. We
investigate the morphological and spectral properties of the radio lobes, the
jets, and the active core. We confirm the co-spatiality of the radio lobes with
the four perpendicular X-ray cavities (see arXiv:2111.03679). The radiative
ages of the E-W lobes ($31.4\pm6.6$ Myr) and of the N-S lobes ($32.1\pm9.9$
Myr) support a coeval origin of the perpendicular outbursts, that also have
similar active phase duration ($\sim$12 Myr). For the inner N-S jets (on scales
of $\leq10$ kpc), we (a) confirm the S-shaped jet morphology; (b) show the
presence of two hotspots per jet with a similar spectral index; (c) estimate
the age of the twisting jets to be less than $\sim8$ Myr. Based on these
results, we determine that jet precession, with period $\sim$9 Myr,
half-opening angle $\sim$24$^{\circ}$ and jet speed $\sim$0.01$c$, can explain
the properties of the N-S jets. We also find that the synchrotron injection
index has steepened from the large, older outbursts ($\Gamma\sim0.5$) to the
younger S-shaped jets ($\Gamma\sim0.9$), possibly due to a transition from an
FR I-like to an FR II-like activity. The VLBI data reveal a single, compact
core at the heart of RBS 797, surrounded by extended radio emission whose
orientation depends on the spatial scale sampled by the data. We explore
several engine-based scenarios to explain these results. Piecing together the
available evidence, we argue that RBS 797 likely hosts (or hosted) binary
active SMBHs. This is still consistent with the detection of a single component
in the VLBI data, since the predicted separation of the binary SMBHs ($\leq$0.6
pc) is an order of magnitude smaller than the resolution of the available radio
data (5 pc).
