We examine the properties of two galaxy ``halos'' at z~0.7 in the Ton 153 (zem=1.01) quasar field. The first absorber-galaxy pair (G1) is a z=0.672, LB=4.3L*B, E/S0 galaxy probed at D=58 kpc. G1 is associated with a remarkable five-component Lyα complex having τLL<=0.4, Wr(Lyα)=2.8 Å, and a velocity spread of Δv=1420 km s-1. We find no Mg II, C IV, N V, nor O VI absorption in these clouds and infer metallicity upper limits of -3<=logZ/Zsolar<=-1, depending on assumptions of photoionized or collisionally ionized gas. The second absorber-galaxy pair (G2) is a z=0.661, LB=1.8L*B, Sab galaxy probed at D=103 kpc. G2 is associated with metal-enriched (logZ/Zsolar~=-0.4) photoionized gas having N(HI)~=18.3 (cm-2) and a velocity spread of Δv=200 km s-1. The very different G1 and G2 systems both have gas-galaxy properties inconsistent with the standard luminosity-dependent galaxy ``halo'' model commonly invoked for quasar absorption line surveys. We emphasize that mounting evidence is revealing that extended galactic gaseous envelopes in the regime of D<=100 kpc do not exhibit a level of homogeneity supporting a standardized halo model. Selection effects may have played a central role in the development of a simple model. We discuss the G1 and G2 systems in the context of ΛCDM models of galaxy formation and suggest that the heterogeneous properties of absorber-galaxy pairs is likely related to the range of overdensities from which galaxies and gas structures arise.