  We want to explore the geometrical structure and mutual interactions of the
innermost components of the broad line radio galaxy (BLRG) 3C 215, with
particular interest in the accretion and ejection mechanisms involving the
central supermassive black hole (SMBH). We compare these observational features
with the ones of the RQ Seyfert 1 galaxies. Investigating their differences it
is possible to understand more about the jet launching mechanisms, and why this
phenomenon is efficient only in a small fraction of all the AGNs. Using high
quality data from a $\sim60$ ks observation with XMM-Newton, we carried out a
detailed X-ray spectral analysis of 3C 215 in the broad energy range $0.5-10$
keV. We modeled the spectrum with an absorbed double power-law model for the
primary continuum, reprocessed by reflection from ionized and cold neutral
material and modified by relativistic blurring. We also compared our results
with the ones obtained with previous multi-wavelength observations. We obtain a
primary continuum photon index from the corona $\Gamma_1=1.97\pm0.06$ and
evidence of a jet contribution, modeled as a power law with photon index
$\Gamma_2\simeq1.29$. The reflector, possibly the accretion disk and portions
of the broad-line region (BLR), is ionized ($\log\xi=2.31_{-0.27}^{+0.37}\
\mathrm{erg\ s^{-1}\ cm}$) and relatively distant from the SMBH ($R_{in}>38\
R_g$), where $R_g=GM_{BH}/c^2$ is the gravitational radius. The obscuring torus
seems patchy, dust-poor and inefficient, while the jet emission shows a twisted
and knotted geometry. We propose three scenarios in order to describe these
characteristics: 1.) ADAF state in the inner disk; 2.) Slim accretion disk; 3.)
sub-pc SMBH binary system (SMBHB).
