In astronomy, what we usually mean by the "size" of a black hole is the extent of its event horizon. For a non-rotating black hole, this is simply:
[tex]R_{BH}=\frac{2GM}{c^2}[/tex]
For a supermassive black hole, this can be as large as the solar system. For a collapsed star, it's a few kilometers. Primordial black holes can be arbitrarily small, perhaps limited by the Planck length. We do expect real black holes to be rotating, but the outer event horizon will still be at the same order of magnitude.