Long-term viscous neutrino-radiation hydrodynamics simulations in full general relativity are performed for a massive disk surrounding spinning stellar-mass black holes with mass M-BH = 4, 6, and 10 M-circle dot and initial dimensionless spin chi approximate to 0.8. The initial disk is chosen to have mass M-disk approximate to 0.1 or 3 M-circle dot as plausible models of the remnants for the merger of black hole-neutron star binaries or the stellar core collapse from a rapidly rotating progenitor, respectively. For M-disk approximate to 0.1 M-circle dot with the outer disk edge initially located at r(out) similar to 200 km, we find that 15%-20% of M-disk is ejected and the average electron fraction of the ejecta is < Y-e > = 0.30-0.35 as found in the previous study. For M-disk approximate to 3 M-circle dot, we find that approximately 10%-20% of M-disk is ejected for r(out) approximate to 200-1000 km. In addition, the average electron fraction of the ejecta can be enhanced to < Y-e > greater than or similar to 0.4 because the electron fraction is increased significantly during the long-term viscous expansion of the disk with high neutrino luminosity until the mass ejection sets in. Our results suggest that not heavy r-process elements but light trans-iron elements would be synthesized in the matter ejected from a massive torus surrounding stellar-mass black holes. We also find that the outcomes of the viscous evolution for the high-mass disk case is composed of a rapidly spinning black hole surrounded by a torus with a narrow funnel, which appears to be suitable for generating gamma-ray bursts.