  In star formation regions, the complex organic molecules (COMs) that contain
peptide bonds ($-$NH$-$C(=O)$-$) play a major role in the metabolic process
because $-$NH$-$C(=O)$-$ is connected to amino acids (R-CHNH$_{2}$$-$COOH).
Over the past few decades, many COMs containing peptide-like bonds have been
detected in hot molecular cores (HMCs), hot corinos, and cold molecular clouds,
however, their prebiotic chemistry is poorly understood. We present the first
detection of the rotational emission lines of formamide (NH$_{2}$CHO) and
isocyanic acid (HNCO), which contain peptide-like bonds toward the chemically
rich HMC G358.93$-$0.03 MM1, using high-resolution and high-sensitivity Atacama
Large Millimeter/submillimeter Array bands 6 and 7. We estimate that the column
densities of NH$_{2}$CHO and HNCO toward G358.93$-$0.03 MM1 are
(2.80$\pm$0.29)$\times$10$^{15}$ cm$^{-2}$ and (1.80$\pm$0.42)$\times$10$^{16}$
cm$^{-2}$ with excitation temperatures of 165 $\pm$ 21 K and 170 $\pm$ 32 K,
respectively. The fractional abundances of NH$_{2}$CHO and HNCO toward
G358.93$-$0.03 MM1 are (9.03$\pm$1.44)$\times$10$^{-10}$ and
(5.80$\pm$2.09)$\times$10$^{-9}$. We compare the estimated abundances of
NH$_{2}$CHO and HNCO with the existing three-phase warm-up chemical model
abundance values and notice that the observed and modelled abundances are very
close. We conclude that NH$_{2}$CHO is produced by the reaction of NH$_{2}$ and
H$_{2}$CO in the gas phase toward G358.93$-$0.03 MM1. Likewise, HNCO is
produced on the surface of grains by the reaction of NH and CO toward
G358.93$-$0.03 MM1. We also find that NH$_{2}$CHO and HNCO are chemically
linked toward G358.93$-$0.03 MM1.
