  We calculate the theoretical event rate of gamma-ray bursts (GRBs) from the
collapse of massive first-generation (Population III; Pop III) stars. The Pop
III GRBs could be super-energetic with the isotropic energy up to $E_{\rm iso}
\gtrsim 10^{55-57}$ ergs, providing a unique probe of the high-redshift
Universe. We consider both the so-called Pop III.1 stars (primordial) and Pop
III.2 stars (primordial but affected by radiation from other stars). We employ
a semi-analytical approach that considers inhomogeneous hydrogen reionization
and chemical evolution of the intergalactic medium. We show that Pop III.2 GRBs
occur more than 100 times more frequently than Pop III.1 GRBs, and thus should
be suitable targets for future GRB missions. Interestingly, our optimistic
model predicts an event rate that is already constrained by the current radio
transient searches. We expect $\sim10-10^4$ radio afterglows above $\sim$ 0.3
mJy on the sky with $\sim 1$ year variability and mostly without GRBs
(orphans), which are detectable by ALMA, EVLA, LOFAR, and SKA, while we expect
to observe maximum of $N < 20$ GRBs per year integrated over at $z>6$ for Pop
III.2 and $N < 0.08$ per year integrated over at $z>10$ for Pop III.1 with
EXIST, and $N < 0.2$ for Pop III.2 GRBs per year integrated over at $z > 6$
with \textit{Swift}.
