  We investigated the thermal evolution of non-spherical primordial gas clouds
of mass $ M=10^6M_\odot $. We studied two cases: 1) prolate and oblate clouds
without angular momentum, 2) initially spherical, oblate and prolate clouds
with angular momentum. In the spherical case, the magnitude of the angular
momentum is the key quantity which determines the fragment mass. The fragment
mass is found to be $M \gsim 100 M_\odot$ for $10^{-2} \lsim \lambda \lsim 1$,
where $\lambda$ is the cosmological spin parameter. For the oblate shape of
initial gas clouds, the angular momentum is almost always not important, In the
case of prolate clouds with some angular momentum, collapse proceeds in the
same way as spherical case, and the bounce occurs to form a disk due to the
angular momentum. In any case, the estimated ``fragment mass'', must be above
$100 M_\odot$ for the primordial gas clouds with typical angular momentum
  and typical oblateness or prolateness.
