  We performed $42$ simulations of the first star formation with initial
supersonic gas flows relative to the dark matter at the cosmic recombination
era. Increasing the initial streaming velocities led to delayed halo formation
and increased halo mass, enhancing the mass of the gravitationally shrinking
gas cloud. For more massive gas clouds, the rate of temperature drop during
contraction, in other words, the structure asymmetry, becomes more significant.
When the maximum and minimum gas temperature ratios before and after
contraction exceed about ten, the asymmetric structure of the gas cloud
prevails, inducing fragmentation into multiple dense gas clouds. We continued
our simulations until $10^5$ years after the first dense core formation to
examine the final fate of the massive star-forming gas cloud. Among the $42$
models studied, we find the simultaneous formation of up to four dense gas
clouds, with a total mass of about $2254\,M_\odot$. While the gas mass in the
host halo increases with increasing the initial streaming velocity, the mass of
the dense cores does not change significantly. The star formation efficiency
decreases by more than one order of magnitude from $\epsilon_{\rm III} \sim
10^{-2}$ to $10^{-4}$ when the initial streaming velocity, normalised by the
root mean square value, increases from 0 to 3.
