  We explore the possibility that the short-lived radionuclides $^{26}$Al,
$^{60}$Fe, $^{107}$Pd, and $^{182}$Hf inferred to be present in the proto-solar
cloud originated from $3-8 M_{\odot}$ Asymptotic Giant Branch (AGB) stars.
Models of AGB stars with initial mass above 5$M_{\odot}$ are prolific producers
of $^{26}$Al owing to hot bottom burning (HBB). In contrast, $^{60}$Fe,
$^{107}$Pd, and $^{182}$Hf are produced by neutron captures: $^{107}$Pd and
$^{182}$Hf in models $\lesssim 5 M_{\odot}$; and $^{60}$Fe in models with
higher mass. We mix stellar yields from solar-metallicity AGB models into a
cloud of solar mass and composition to investigate if it is possible to explain
the abundances of the four radioactive nuclides at the Sun's birth using one
single value of the mixing ratio between the AGB yields and the initial cloud
material. We find that AGB stars that experience efficient HBB ($\geq 6
M_{\odot}$) cannot provide a solution because they produce too little
$^{182}$Hf and $^{107}$Pd relative to $^{26}$Al and $^{60}$Fe. Lower-mass AGB
cannot provide a solution because they produce too little $^{26}$Al relative to
$^{107}$Pd and $^{182}$Hf. A self-consistent solution may be found for AGB
stars with masses in-between ($4-5.5 M_{\odot}$), provided HBB is stronger than
in our models and the $^{13}$C($\alpha$, n)$^{16}$O neutron source is mildly
activated. If stars of M $< 5.5 M_{\odot}$ are the source of the radioactive
nuclides, then some basis for their existence in proto-solar clouds needs to be
explored, given that the stellar lifetimes are longer than the molecular cloud
lifetimes.
