We investigate explosive nucleosynthesis in a delayed neutrino-driven, supernova explosion aided by standing accretion shock instability (SASI), based on two-dimensional hydrodynamic simulations of the explosion of a 15M⊙ star. We take into accounts neutrino heating and cooling as well as change in electron fraction due to weak interactions appropriately, in the two-dimensional simulations. We assume the isotropic emission of neutrinos from the neutrino spheres with given luminosities. and the Fermi-Dirac distribution of given temperatures. We find that the stalled shock revives due to the neutrino heating aided by SASI for cases with Lν e ≥ 3.9 × 1052ergs s-1 and the aspherical shock passes through the outer layers of the star (≥ 10,000 km), with the explosion energies of ∼ 1051ergs. Next we examine abundances and masses of the supernova ejecta. We find that masses of the ejecta and 56Ni correlate with the neutrino luminosity, and 56Ni mass is comparable to that observed in SN 1987A. We also find that abundance pattern of the supernova ejecta is similar to that of the solar system, for cases with high explosion energies of > 1051ergs. We emphasize that 64Zn, which is underproduced in the spherical case, is abundantly produced in slightly neutron-rich ejecta.