  We present theoretical yields of H, $^{4}$He, $^{12}$C, $^{13}$C, $^{14}$N,
and $^{16}$O for stars with initial masses between 0.8 and 8 M$_{\odot}$ and
initial metallicities Z = 0.001, 0.004, 0.008, 0.02, and 0.04. We use the
evolutionary tracks of the Geneva group up to the early asymptotic giant branch
(AGB) in combination with a synthetic thermal-pulsing AGB evolution model to
follow in detail the chemical evolution and mass loss up to the end of the AGB
including the first, second, and third dredge-up phases. Most of the relations
used are metallicity dependent to make a realistic comparison with stars of
different initial abundances. The effect of Hot Bottom Burning (HBB) is
included in an approximate way. The free parameters in our calculations are the
mass loss scaling parameter $\eta_{AGB}$ for stars on the AGB (using a Reimers
law), the minimum core mass for dredge-up M$_{c}^{min}$, and the third
dredge-up efficiency $\lambda$. As derived from previous extensive modeling,
$\eta_{AGB}$ = 4, M$_{c}^{min}$ = 0.58 \mss, and $\lambda = 0.75$ including HBB
are in best agreement with observations of AGB stars both in the Galactic disk
and the Magellanic Clouds. We compare the abundances predicted during the final
stages of the AGB with those observed in planetary nebulae in the Galactic disk
and show that the model with the aforementioned parameters is in good agreement
with the observations. The metallicity dependent yields of intermediate mass
stars presented in this paper are well suited for use in galactic chemical
evolution models.
