We present a long ( 116 ks ) Suzaku observation of the Broad-Line Radio Galaxy ( BLRG ) 3C 382 acquired in April 2007 . A Swift BAT spectrum in 15–200 keV from the 58-month survey is also analyzed , together with an archival XMM-Newton EPIC exposure of 20 ks obtained one year after Suzaku . Our main result is the finding with Suzaku of a broad Fe K line with a relativistic profile consistent with emission from an accretion disk at tens of gravitational radii from the central black hole . The XIS data indicate emission from highly ionized iron and allow us to set tight , albeit model-dependent , constraints on the inner and outer radii of the disk reflecting region , r _ { in } \simeq 10 r _ { g } and r _ { out } \simeq 20 r _ { g } , respectively , and on the disk inclination , i \simeq 30 ^ { \circ } . Two ionized reflection components are possibly observed , with similar contributions of \sim 10 % to the total continuum . A highly ionized one , with log \xi \simeq 3 erg s ^ { -1 } cm , which successfully models the relativistic line and a mildly ionized one , with log \xi \simeq 1.5 erg s ^ { -1 } cm , which models the narrow Fe K \alpha and high energy hump . When both these components are included , there is no further requirement for an additional black body soft excess below 2 keV . The Suzaku data confirm the presence of a warm absorber previously known from grating studies . After accounting for all the spectral features , the intrinsic photon index of the X-ray continuum is \Gamma _ { x } \simeq 1.8 with a cutoff energy at \sim 200 keV , consistent with Comptonization models and excluding jet-related emission up to these energies . Comparison of the X-ray properties of 3C 382 and other BLRGs to Seyferts recently observed with Suzaku and BAT confirms the idea that the distinction between radio-loud and radio-quiet AGN at X-rays is blurred . The two classes form a continuum distribution in terms of X-ray photon index , reflection strength , and Fe K line width ( related to the disk emission radius ) , with BLRGs clustered at one end of the distribution . This points to a common structure of the central engine , with only a few fundamental parameter ( s ) responsible for the radio-loud/radio-quiet division . The black hole spin , and in particular its rotation compared to the disk ’ s , may be a key one .