  Detecting and modelling the reprocessed hard X-ray emission component in the
accretion flow, so-called reflection spectrum is a main tool to estimate black
hole spins in a wide range of astrophysical black holes regardless of their
mass or distance. In this work, we studied the X-ray spectra of the Seyfert I
galaxy III Zw 2 using multi-epoch XMM-Newton, NuSTAR and Suzaku observations.
The X-ray spectra exhibit a soft-excess below 1 keV and a prominent excess at
the location of the broad Fe K{\alpha} line at 6.4 keV. To account for these
spectral features, we have fitted the spectra with multiple models including an
ionized partially covering absorber and an accretion disk reflection model. To
fully resolve the reflection component, we analyzed jointly the XMM-Newton and
NuSTAR observations taken in 2017 and archival XMM-Newton data from 2000.
Assuming the reflection scenario, the resulting model fits support a rapidly
spinning black hole (a > 0.98) in this radio-intermediate source. The X-ray
spectra in 2000 and 2017 are remarkably similar with the only difference in the
reflection fraction, possibly due to a change in the geometry of the accretion
flow. However, the Suzaku observation is markedly different, and we suggest
this could be an effect of a jet contribution in the X-ray band, which is
supported by the elevated radio flux during this observation.
