The Hungaria region is located at the inner edge of the asteroid main belt (at semi-major axis a < 2 AU), and it is located at high inclinations and low to moderate eccentricities.  The limitations in eccentricity allow for a perihelion large enough to avoid strong interactions with Mars, even considering secular changes in the Mars eccentricity.  (Milani et al. 2010).  The g-g₃ and g-g₅ secular resonances fix the dynamical limits of the Hungaria region in inclination. Only one family has been so far positively identified in the Hungaria orbital region, the namesake (434) Hungaria group by
Milani et al. (2010).  Other authors (Cañada-Assandri et al. 2013) pointed out that the highly inclined Hungaria population is dominated by S-type objects, and fairly distinguished from the C-complex population observed in the Hungaria dynamical family.   But no family in proper elements domain has yet been observed in this highly inclined region.  We identified only 37 objects in our multi-domain sample, with reasonable errors, and two possible families, reported in the table.   Asteroids in the Hungaria region tend to have high albedo values, as shown in the Fig. 3.