Yes, the existing data is very poor, after reading up on Pop-III stars. They are in fact hypothetical, and deemed (by many) to have been formed exclusively as super giants, with 100s of SMs. Other concepts put them in a range of sizes, with some of them still existing today. It seems that this is all based on metallicity.
I recall reading, not sure where, that some smaller stars could have formed very early, during the formation of Pop-III stars, and that a few of them still exist. Seem to recall that one super-low metallicity star was observed in a binary in the Milky Way, but don't recall the details.
There is no proof that the earliest stars (Pop-III) were all super-giants and now long gone. Was surprised to hear that there are none in globular clusters, but then that observation may simply be defined as size, rather then metallicity? How can you measure the metallicity of all (e.g.) 100,000 stars in a cluster?
I do recall the formation of blue stars in globular clusters (GCs), by the fusion of two old yellow stars. The combined mass of hydrogen was enough to light them up as blue giants. Is it possible that some of the stars in GCs are actually fused Pop-III stars that started smaller than models suggest they should?
It seems likely that there are a few Pop-III stars out there that are low mass and long-lived. If so, they would offer unique opportunities to study the earliest stars.