We present extensively dense observations of the super-Chandrasekhar supernova (SC SN) candidate SN 2012dn from \(-11\) to \(+140\) days after the date of its \(B\)-band maximum in the optical and near-infrared (NIR) wavelengths conducted through the OISTER ToO program. The NIR light curves and color evolutions up to 35 days after the \(B\)-band maximum provided an excellent match with those of another SC SN 2009dc, providing a further support to the nature of SN 2012dn as a SC SN. We found that SN 2012dn exhibited strong excesses in the NIR wavelengths from \(30\) days after the \(B\)-band maximum. The \(H\) and \(K_{s}\)-band light curves exhibited much later maximum dates at \(40\) and \(70\) days after the \(B\)-band maximum, respectively, compared with those of normal SNe Ia. The \(H\) and \(K_{s}\)-band light curves subtracted by those of SN 2009dc displayed plateaued evolutions, indicating a NIR echo from the surrounding dust. The distance to the inner boundary of the dust shell is limited to be \(4.8 - 6.4\times10^{-2}\) pc. No emission lines were found in its early phase spectrum, suggesting that the ejecta-CSM interaction could not occur. On the other hand, we found no signature that strongly supports the scenario of dust formation. The mass loss rate of the pre-explosion system is estimated to be \(10^{-6}-10^{-5}\) M\(_{\odot}\) yr\(^{-1}\), assuming that the wind velocity of the system is \(10-100\) km~s\(^{-1}\), which suggests that the progenitor of SN 2012dn could be a recurrent nova system. We conclude that the progenitor of this SC SN could be explained by the single-degenerate scenario.