  We present an analysis of the spectral energy distribution (SED) of the
galaxy ESO 184-G82, the host of the closest known long gamma-ray burst (GRB)
980425 and its associated supernova (SN) 1998bw. We use our observations
obtained at the Australia Telescope Compact Array (the third >3 sigma radio
detection of a GRB host) as well as archival infrared and ultraviolet (UV)
observations to estimate its star formation state. We find that ESO 184-G82 has
a UV star formation rate (SFR) and stellar mass consistent with the population
of cosmological GRB hosts and of local dwarf galaxies. However, it has a higher
specific SFR (per unit stellar mass) than luminous spiral galaxies. The mass of
ESO 184-G82 is dominated by an older stellar population in contrast to the
majority of GRB hosts. The Wolf-Rayet region ~800 pc from the SN site
experienced a starburst episode during which the majority of its stellar
population was built up. Unlike that of the entire galaxy, its SED is similar
to those of cosmological submillimeter/radio-bright GRB hosts with hot dust
content. These findings add to the picture that in general, the environments of
GRBs on 1-3 kpc scales are associated with high specific SFR and hot dust.
