  We explore the possibility that the recently detected black hole binary (BHB)
merger event GW190521 originates from the first generation of massive,
metal-free, so-called Population III (Pop III), stars. Based on improved binary
statistics derived from N-body simulations of Pop III star clusters, we
calculate the merger rate densities of Pop III BHBs similar to GW190521, in two
evolution channels: classical binary stellar evolution and dynamical hardening
in high-redshift nuclear star clusters. Both channels can explain the observed
rate density. But the latter is favoured by better agreement with observation
and less restrictions on uncertain parameters. Our analysis also indicates that
given the distinct features of the two channels (with merger rates peaked at
$z\lesssim2$ and $z\sim 10$, respectively), future observation of BHB mergers
similar to GW190521 with third-generation gravitational wave detectors will
greatly improve our knowledge of the evolution of Pop III BHBs, especially for
their dynamics during cosmic structure formation.
