  Most Vega-like stars have far-infrared excess (60micron or longward in IRAS,
ISO, or Spitzer MIPS bands) and contain cold dust (<~150K) analogous to the
Sun's Kuiper-Belt region. However, dust in a region more akin to our asteroid
belt and thus relevant to the terrestrial planet building process is warm and
produces excess emission in mid-infrared wavelengths. By cross-correlating
Hipparcos dwarfs with the MSX catalog, we found that EF Cha, a member of the
recently identified, ~10 Myr old, ``Cha-Near'' Moving Group, possesses
prominent mid-infrared excess. N-band spectroscopy reveals a strong emission
feature characterized by a mixture of small, warm, amorphous and possibly
crystalline silicate grains. Survival time of warm dust grains around this A9
star is <~ 1E5 yrs, much less than the age of the star. Thus, grains in this
extra-solar terrestrial planetary zone must be of "second generation" and not a
remnant of primodial dust and are suggestive of substantial planet formation
activity. Such second generation warm excess occurs around ~ 13% of the
early-type stars in nearby young stellar associations.
